cusp structures and magnetic reconnection at the...
TRANSCRIPT
Cusp Structures and
Magnetic Reconnection
at the Magnetopause
JACQUELINE JENSENUNIVERSITY OF CENTRAL FLORIDA
LASP BOULDER, CO
MENTOR: KARLHEINZ TRATTNER
Why Study Magnetic
Reconnection? Fundamental process
Sun: Solar Flares, CMEs, Flare Loops
Earth: Plasma Entry, Auroras, Magnetic storms
Ultimate Goal: Observe
magnetic reconnection in
situ through predictions of
reconnection site in model
Magnetic
Reconnection
The Magnetosphere
Solar wind: made up of plasma particles. Field distortion caused by pressure
Bow shock: shock wave before Earth’s magnetic field
Magnetosheath: region of higher density shocked plasma
Magnetopause: Boundary between the solar wind and Earth’s magnetic field
Cusp region: region with open field lines and direct solar wind access to upper atmosphere
Reconnection at the
Magnetopause
Plasma Entry
Precipitating cusp ions experience a velocity filter effect with lower
energies
convecting further poleward
Instrument Overview
Polar’s TIMAS Instrument
Mass spectrometer
Collects data on He+, He++, O+, and H+
Focused on H+ data
Measures 3D velocity
distributions
TIMAS Schematic
Southward IMF
Reconnection
Northward IMF
Reconnection
Southward IMF
Northward IMF
Not Just When, But
Where? Maximum Magnetic Shear Model
Predicts where reconnection is most likely to
occur
Correct 80% of the time
Shear angle plot:
Angle between solar wind magnetic field
and earth’s magnetic field lines
IMF clock angle:
Organizational
parameter for plots
Maximum Magnetic Shear
Magnetospheric Multiscale
Mission (MMS)
Anomalies
Observed: 176.1°
ACE: 112.5°
Observed: 153.5°
WIND: 132.8°
Observed: 50.3°
ACE: 80.0 °
Observed: 151.4°
ACE: 127.9°
Modeling the X-Line
• Ions are reflected when they
reach the ionosphere
• Xm = Distance to ionospheric
mirror point, calculated using
Tsyganenko 1996 model
(known value)
• Vm = cutoff velocity of
mirrored ions
• Ve = cutoff velocity of
earthward propagating ions
(precipitating)
• Xr = distance to reconnection
point (Calculated by program)
Modeling X-Line Part 2
• TIMAS data is
presented in a field-aligned coordinate system
• Gaussian distributions are fitted to the peaks
• Cutoff velocities are determined from Gaussian fits
Reconnection X-Line
Clock Angle 200-260
Anomalies arise between 200° and 260°
Occurs all year but predominately in spring time
Unknown why anomalies occur within this range
Data and Trends •58 events analyzed
•No events in main duration of winter
and summer
•Most events occurring in spring
Data and Trends
Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Total
Events 0 0 14 13 14 5 0 0 3 7 2 0 58
Above 0 0 9 5 0 0 0 0 0 1 0 0 15
Below 0 0 1 3 10 2 0 0 1 5 2 0 24
On Target
0 0 4 5 4 3 0 0 2 1 0 0 19
• 32.8% on target with model
• Predominately above in March
• Even statistics in April
• Predominately below after April
• Statistics for Bx value were
even
• Distribution of Clock Angles
was even
Conclusion
March events occur predominately above the
predicted x-line
April statistics are about even
All months after April seem to occur below the predicted x-line
April seems to be the turning point for this change
No other parameter yielded any trends
Future
Investigation
Plot more events
within this range
Does the pattern still occur?
Investigate other
Magnetopause parameters
Alfven Velocity
Plasma Beta
Questions?
Acknowledgements and
References
1. Trattner, K.J., S. A. Fuselier, and
S. M. Petrinec. “Location of the
reconnection line for northward
interplanetary magnetic field.”
J. Geophys. Res. 109 (2004)
This research was funded
by the National Science
Foundation under grand
number 1659878, as part
of a Research Experience
for Undergraduates at
the University of Colorado
at Boulder.
All pictures courtesy of
NASA. All plots and
spectrograms were
produced using an IDL
program written by
Karlheinz Trattner.